... To be read in conjunction with Section 4.11 of the WFPC2 Instrument Handbook , -Version 4.0. ... 1 The second study found evidence that CTE loss for faint stars has increased with time (Whitmore, 1998). The primary observational consequence of CTE loss is that a point source at the top of the chip appears to be fainter than if observed at the bottom of the chip, due to the loss of electrons as the star is read out down the chip (see Figure 1 ). ... Last updated: 06/16/98 10:38:00 . ...

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• Further Investigations
• Results and Discussions
• Thermal/Sky Backgrounds GPI Data Pipeline 1.0 documentation

These observations are aimed at fully charactering FORS1 photometric system (UBVRI zero-points, color-terms and extinction coefficients) for the Tektronix 2048x2048 pixel CCD (24µm px) . To this aim, the two Landolt/Stetson photometric fields SA95 and SA101 will be observed on a number of epochs and at different airmasses during February and March 2007. ... SA101 . ... OBs for SA101 have to be observed during evenigh twilight (exceptions are expected for the second half of March) . ...

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• Homepage of Christian A. Hummel
• Titan Observed Through Nine Different Filters on November 26, 2002 | ESO
• Titan Observed Through Nine Different Filters on November 26, 2002 | ESO United

Observed maximum rotation velocity uncorrected for inclination effect. This quantity is calculated from 21-cm line widths at different levels and/or rotation curves (generally in H_alpha). ... These data are characterized by some secondary parameters: telescope, velocity resolution, level of the 21-cm line width and bibliographic reference. ... we start from a standard sample (a set of measurements giving a large and homogeneous sample). ... HyperLeda . ...

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• Equations of condition
• Getting the observations
• Optical spectroscopy

... the time of observation . ... Observing the Changing Position of the Sun To Establish Cardinal Directions . ... Observations of the Sun's apparent movement across the sky and its pattern of rising and setting in the east and west horizon helped to establish the cardinal directions. ... The final stage of the Sun's return was marked by the observation that the Sun had reached its highest altitude when the full width of your mitted hand could fill the gap between the Sun and the horizon. ...

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• ASP: An Ancient Universe - Changes in Stars

Next: Description Up: OM Related CCF Components Previous: Generation from In-Orbit Data Contents . The analysis of calibration observations of fields observed in different positions of the detector has demonstrated that large sensitivity variations do not exist in OM data, or they are smaller than the errors of the photometry (a few percent). ... Something similar occurs with pixel to pixel variations (see 4.5.9 ). ... Generation from Ground Calibration Data . Generation from In-Orbit Data . ...

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• XMM Science Objectives
• Description
• Observing mode support

ARCSAT ID NUMBER: AS07 DESCRIPTIVE TITLE: Short Term Variability for Stars of Similar Temperatures but Different Luminosities PI: Tiffany Pewett (GSU) OBSERVER(S): Tiffany Pewett (GSU), Michele Silverstein (GSU), Todd Henry (GSU) UNCERTIFIED/UNTRAINED OBSERVERS: COLLABORATORS: Wei-Chun Jao (GSU) CONTACT INFORMATION: Tiffany Pewett, pewett@astro.gsu.edu, 419-460-0072 TIME REQUESTED: 7 nights 1. ... FEB 09-15 7 nights are requested to observe ~14 stars for photometric variability. ...

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• http://www.apo.nmsu.edu/Telescopes/ARCSAT/ObsSchedules/arcsat_apr2016/AS04.html
• http://www.apo.nmsu.edu/Telescopes/ARCSAT/ObsSchedules/arcsat_oct2015/AS08.html
• http://www.apo.nmsu.edu/Telescopes/ARCSAT/ObsSchedules/arcsat_jan2016/AS04.html

... In order to compare the number of different evolutionary stages obtained and X-ray luminosity of the chosen X-ray sources with the observed galactic values we use the sum of C/O+O/C , where C and O are the calculated and observed values of a given binary type, respectively. If we make comparison for a number of different binary species (for example, we compare the number of CV, number of X-ray pulsars,   total X-ray luminosity of LMXB, etc.), we write this criterion in the form: . ...

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• Evolution of the Double Neutron Star Merging Rate andthe Cosmological Origin of
• Gravitational waves from supernova explosions
• Introduction

Next: Radial velocity of the Up: Optical spectrum of IRAS04296 Previous: Observations and spectra reduction . ... However, molecular emission features are only very rarely observed in the optical spectra of PPNe. ... On the other hand, it is well known that cometary nuclei spectra show prominent Swan band emission. In both spectra of IRAS04296 we have discovered strong emission in the (0;0) and (0;1) bands of the Swan system of the molecule. ... Now consider the case of IRAS04296. ...

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• di_eks
• These galaxies were observed (Project: vortex)
• SCORPIO: IFP Gallery

The potential of masers to act as probes of their environment has long been recognised, but to date has proven very difficult to realise. ... 2001, Sutton et al. 2001). Masers are variable on timescales of weeks to months and one of the major limitations in previous attempts at multi-transition analysis has been the uncertainties introduced by combining observations made over many years using a variety of instruments with differing spectral and spatial resolutions and polarisation properties. ...

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• Australia Telescope Compact Array Home Page
• Source size measurement from observed quasar microlensing
• DOPSRC

Next: C.S. Jeffery, Research Astronomer Up: Research Previous: J.E. Chambers, Research Astronomer Contents . During 1998 Dr Gerry Doyle was involved with three PPARC PDRA research grants, and was also a co-organiser of two international conferences (the COSPAR Symposium `Activity Observed in the Sun and in Similar Stars', and the Armagh Cool Star Workshop `Solar and Stellar Activity: Similarities and Differences'). He was Associate Scientist with the CDS and SUMER instruments on SOHO. ...

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• Armagh Astronomers to observe Ringing Star with Global Telescope
• Armagh Observatory
• Broadening of Si VIII lines observed in the Solar polar coronal holes

... The first task assumes the searching for chemical composition and sizes of particles which give the wavelength dependence of the extinction efficiencies close to the observed dependence of . Figure 7: Wavelength dependence of the extinction efficiency factors for homogeneous spherical particles of different sizes consisting of astronomical silicate and amorphous carbon. The dashed segment shows the approximate wavelength dependence of the mean galactic extinction curve at optical wavelengths. ...

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• Linear polarization: wavelength dependence
• Extinction properties (transmitted radiation)
• Footnotes

This is a list of all currently available observing modes in CIMA. Different modes are available depending on whether CIMA is run in pulsar or in spectral line mode. ... Note that the appearance of the windows refer to CIMA version 3.1 , which for most observing modes is slightly different than from CIMA version 2.3 and 3.0 and completely different from CIMA version 2.2. ... Non-ALFA . ... Pulsar cross calibration . ... Drift map . ... ALFA : indicates whether the observing mode works with ALFA . ...

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• CIMA Auto-Observing
• CIMA Frequently Asked Questions
• observing techniques

... Under certain conditions, like those in the nucleus of a QSO, all atoms can be made to emit light at particular wavelengths. ... If that source is approaching the observer, the wave is squashed up onto itself making the wavelength shorter. ... This is redshift. ... You can see how the section of the QSO spectrum which we observe changes with redshift. ... We then see how far we had to slide the observed spectrum along the scale to make it match and that is the objects redshift. ... The 2QZ team . ...

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The problem of solar wind data correlation for the observations onboard several spacecraft is very important for three points of view: . ... This problem is studied now in detail by systematic determination of ion flux and ion velocity data correlations by INTERBALL-1 (IKI group), WIND and IMP 8 (both - MIT group). ... Solar wind plasma correlation lengths from IMP 8, WIND and INTERBALL-1. ... Correlation of solar wind observations onboard several spacecraft: INTERBALL-1, IMP 8 and WIND data. ...

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• Seasons of the Year
• Space Research Institute (IKI) Seminar
• Spacecraft Observing the Sun and the Heavens above

M. ( / DIAS, Ireland), A. (ISDC, Switzerland) 1 - Key Question Only 3 binary systems regularly observed in TeV: PSR B1259-63 (young pulsar +Be star, P=3.4 y) LSI +61 303 (comp. source + Be star, P=26.42 d) LS 5039 (comp. source + O star, P=3.9 d) Origin of the high-energy emission? ... 2006; Neronov &Chernyakova 2007 4 3.4 years orbital period. e~0.87 Correlated variability with a sharp rise ( "two bumps structure" ) is seen in radio, X-ray (and TeV?) bands. ...

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• Fast search through RTT150 data archive
• GRANAT Home Page

... Does the time it takes different methods to create all the elements coincide with the universeт??s accepted age? ... Illinois Urbana-Champaign) Different kinds of stars create elements at different rates, all of which are consistent with the age of the universe. Get instant access to subscriber content on Astronomy.com! ... Registration is FREE and takes only a few seconds to complete. If you are already registered on Astronomy.com, please log in below. ...

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• Why do some stars appear to flash a variety of different colors when you look
• Magnetic fields, subatomic particles, etc., traveling in different directions
• The Sun has an 11-year sunspot cycle. Do we know if other stars have similar

IBIS Data Analysis . ... IBIS . ... Flat Fielding - Introduction . The images obtained by IBIS will have intensity variations across the field of view that are not due to the solar image, but rather caused by instrumental effects that alter the observed intensity in each point of the field of view. ... IBIS Flat Fielding Techniques . ... Therefore, it is desirable to obtain the flat field measurements center on a point along the equator near the heliographic center of the solar disk. ...

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• Observing capabilities
• Clumpy dust disks
• The Discovery of the Galilean Satellites

... Yes, but how many dark clouds have a multicolored lining? Pictured, behind this darker cloud, is a pileus iridescent cloud, a group of water droplets that have a uniformly similar size and so together diffract different colors of sunlight by different amounts. ... TrES 2b: Dark Planet . ... Planet TrES-2b reflects back less than one percent of the light it receives, making it darker than any known planet or moon, darker even than coal. ... The Fairy of Eagle Nebula . ... Next [ Last page ] . ...

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• Journal "Peremennye Zvezdy"
• Hale-Bopp and the Plateau de Bure Interferometer
• Астронет > Hale-Bopp and the Plateau de Bure Interferometer

January 7, 2000 Dr. Eric Torrence, University of Chicago . ... 3:00pm, 240D Willamette Hall . Dr. Torrence will also present the Physics Colloquium on January 6. return to top . ... Dr. Morii will also present the Physics Colloquium on January 24. return to top . ... return to top . ... The ratio of the inclusive jet cross sections at center of mass energies 0.63 TeV and 1.8 TeV is also presented versus scaled jet transverse energy x_T and compared to QCD predictions. 3:00pm, 472 Willamette Hall . ...

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• Astro-2 and the UIT Experiment
• Venus and Mars

... The extinction in terrestrial atmosphere. ... A star was observed at different zenith distances during one night at the Engelgardt's Astronomical Observatory in the program of atmospheric extinction study at blue. ... Calculate the air mass for given zenith distances in 1st 54.9 11800 column, and write the result into the 2nd column. ... Spectral observations. ... Calculate the radial velocity Vr of the star on each date, the results of measurements and write calculations into the table. ...

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• http://www.issp.ac.ru/iao/2015/booklet/b10_ia15_p_en_a.pdf
• http://www.issp.ac.ru/lhpp/PapersBashkin/117e.pdf
• http://www.issp.ac.ru/lhpp/PapersAntonov/92.pdf